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IAUC 7687: 2001 Q2; N Cyg 2001 No. 2; CI Aql

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                                                  Circular No. 7687
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
URL http://cfa-www.harvard.edu/iau/cbat.html  ISSN 0081-0304
Phone 617-495-7440/7244/7444 (for emergency use only)

COMET 2001 Q2
     Additional astrometry by P. Pravec and P. Kusnirak with the
Ondrejov 0.65-m f/3.6 reflector + CCD:

     2001 UT             R.A. (2000) Decl.
     Aug. 20.07522    5 41 32.03   +27 34 34.1
          20.08395    5 41 35.00   +27 34 23.6

     Visual m_1 estimates:  Aug. 20.09 UT, 10.4 (R. J. Bouma,
Groningen, The Netherlands, 0.25-m reflector); 20.31, 10.8 (P. M.
Raymundo, Salvador, Brazil, 0.15-m refractor).
     Corrigenda.  On IAUC 7686, lines 2 and 12, FOR  Cyprus Hills,
READ  Cypress Hills Interprovincial Park,

NOVA CYGNI 2001 No. 2
     S. Nakano, Sumoto, Japan, reports the independent discovery of
this nova (cf. IAUC 7686) by K. Hatayama (Niigata, Japan) on two
1-min exposures taken on Aug. 18.625 UT with a 100-mm f/5.6 camera
lens and Fuji Superia 400 film that show the nova at mag 7.0
(limiting mag 10).  Nothing was visible at this position on
Hatayama's films taken on 2000 Sept. 29, Oct. 22, 2001 July 21, and
July 25.  T. Kato, Kyoto University, reports the following limiting
magnitudes (nova not seen) from unfiltered CCD images:  Aug. 2.654,
[13.2 (A. Takao, Kitakyushu, Japan); 11.520, [14.3 (Y. Sano,
Nayoro, Japan); 12.699, [14.1 (Takao); 17.628, [14.1 (Takao).
     CCD photometry by G. Sostero and A. Lepardo, Remanzacco,
Italy (0.3-m Baker camera):  Aug. 19.84 UT, V = 6.66, B-V = +1.1,
V-R_c = +0.5, R_c-I_c = +0.9.  CCD photometry by J. D. West,
Mulvane, KS (0.25-m refl.):  Aug. 20.098, V = 6.89; 20.138, V =
7.08; 20.087, I_c = 4.48.

     B. E. Schaefer, University of Texas at Austin, writes:  "The
recurrent nova CI Aql has now faded back to near its normal
quiescent state with an eclipsing light curve varying from V = 15.3
to 16.2, as seen from Aug. 4.1 to 10.3 UT with the 2.1-m telescope
at McDonald Observatory.  This implies that the system is no longer
a supersoft x-ray source and that the hydrogen content of the white
dwarf envelope is X about 0.4 (Hachisu and Kato,
http://xxx.lanl.gov/abs/astro-ph/0104461).  The formerly prominent
secondary minimum is no longer visible; instead, the magnitude
fades linearly by 0.10 mag between phases 0.35 and 0.65."

                      (C) Copyright 2001 CBAT
2001 August 20                 (7687)            Daniel W. E. Green

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